! File: 4128C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:09:51:35 coverpage: title_1: GRAVITATIONALLY LENSED QSOS: title_2: CYCLE 9 OBSERVATIONS sci_cat: QUASARS & AGN sci_subcat: GTO/FOS proposal_for: GTO/FOS cont_id: 1030 pi_fname: E. MARGARET pi_lname: BURBIDGE pi_inst: UNIVERSITY OF CALIFORNIA, SAN DIEGO pi_country: USA pi_phone: 619-534-4477 keywords_1: GRAVITATIONAL LENSES, QUASARS, UV ABSORPTION LINES. hours_pri: 11.07 num_pri: 3 fos: Y ! end of coverpage abstract: line_1: This proposal contains observations which will help to complete a number of FOS line_2: IDT scientific programs. Evolution of the sizes of the Lyman line_3: alpha clouds will be studied with ultraviolet spectra of a well separated pair line_4: of QSO images. line_5: In two "gravitational lensing" multiple QSOs, we shall ascertain line_6: whether the UV spectra of the images are identical, while detecting line_7: absorption lines (especially Lyman alpha) which might exhibit differences and line_8: hence give information on sizes of absorbing clouds. ! ! end of abstract general_form_proposers: lname: HARMS fname: RICHARD mi: J. inst: APPLIED RESEARCH CORPORATION country: USA ! lname: ALLEN fname: RICHARD mi: G. inst: UNIVERSITY OF ARIZONA country: USA ! lname: ANGEL fname: J. ROGER mi: P. inst: UNIVERSITY OF ARIZONA country: USA ! lname: BARTKO fname: FRANK inst: UNAFFILIATED country: USA ! lname: BEAVER fname: EDWARD inst: UC, SAN DIEGO country: USA ! lname: BOHLIN fname: RALPH mi: C. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: BURBIDGE fname: E. MARGARET title: PI inst: UC, SAN DIEGO country: USA ! lname: COHEN fname: ROSS mi: D. inst: UC, SAN DIEGO country: USA ! lname: DAVIDSEN fname: AURTHUR mi: F. inst: JOHNS HOPKINS UNIVERSITY country: USA ! lname: FORD fname: HOLLAND mi: C. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: HARTIG fname: GEORGE mi: F. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: JUNKKARINEN fname: VESA mi: T. inst: UC, SAN DIEGO country: USA ! lname: MARGON fname: BRUCE mi: H. inst: UNIVERSITY OF WASHINGTON country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The two brightest components of PG1115+080 will be observed with the line_2: FOS Red detector and 0.3" aperture. For each observation a binary line_3: search will be done on an offset star, followed by a move to the line_4: object. There will be a an ACQ image, followed by spectra with G400H line_5: (2400 and 3100 seconds), G270H (5050 and 6820s), and G190H (5074 and line_6: 7337s). ! question: 4 section: 1 line_1: The Lyman-alpha forest lines in the spectrum of two components of line_2: PG 1115+080 for measuring the size of the H I clouds are below the line_3: atmospheric cutoff. Absorption lines such as C IV lambda1549 due to line_4: low and medium redshift galaxies and galaxy clusters near QSO sight line_5: lines will be in the UV. UV absorption lines are a better probe of gas line_6: for this sight lines than optical absorption lines, and the UV line_7: observations are required in order to understand the evolution of the line_8: sizes of these clouds. ! question: 4 section: 2 line_1: The collecting area of HST and the sensitivity of the FOS and GHRS line_2: make it possible to obtain spectra with the signal to noise needed to line_3: carry out these studies of QSOs at wavelengths below the atmospheric line_4: cutoff. ! question: 7 section: 1 line_1: Absorption lines in the spectra of the line_2: two gravitational lens images will be measured using the standard line_3: software. Monte-Carlo simulations of the absorption line coincidences line_4: along these two closely spaced lines of sight will be used to estimate line_5: the size of the Ly-alpha forest H I clouds. The association of line_6: absorption lines with galaxies and clusters of galaxies along the QSO line_7: line of sight will be established by obtaining accurate redshifts for line_8: the absorption system and the intervening object. ! question: 7 section: 2 line_1: These observations will be reduced using the standard spectroscopy line_2: reduction software available for FOS data. Calibration line_3: will be done using the results of SV observations. line_13: The absorption features in QSO spectra will be measured using existing line_14: software that has been used for optical data and the early HST line_15: spectra. The evolution of C IV lambda1549 absorption systems with line_16: redshift will be studied by counting these systems and carrying out line_17: the necessary statistical analysis. Unidentified lines below line_18: Ly-alpha emission are candidate Ly-alpha forest lines and will line_19: contribute to studies of the evolution of these absorbers. Metal line line_20: systems will be studied by using curves of growth to obtain estimates line_21: and limits to column densities. ! question: 8 section: 1 line_1: line_2: Optical spectroscopy and line_3: photometry will be performed using the facilities of Lick Observatory. line_4: We will try to make the optical observations simultaneous with the line_5: HST UV observations if possible. This imposes no requirements on HST. line_7: Coordinates need to be determined from WF/PC team images for line_8: target acquisition. line_10: There are a number of related FOS IDT GTO proposals in cycles 0, 1, line_11: and 2. These observations were originally written as portions line_12: of observations begun in those proposals. Thus the observations line_13: included here contain both the baseline and augmented portions. Some line_14: observations were moved from augmented to baseline proposals to line_15: balance this. ! question: 9 section: 1 line_1: Collaborators have received data from a number of GTO programs, SAT, line_2: and ERO programs. Related programs which have had observations are as line_3: follows: line_4: 1026 - ``UV Spectra of Low-Redshift-QSOs'', line_5: 1027 - ``UV Spectra of QSOs with z> 3.1'', line_6: 1029 - ``Spectropolarimetry of QSOs, Blazars, and AGN'', and line_7: 1033 - ``Search for Misdirected BL Lac Objects''. line_8: Low resolution observations of three high redshift QSOs have not line_9: revealed any with light at He II lambda 304. Observations of UM 675 line_10: have shown that any He I Gunn--Peterson effect is small, that He I line_11: absorption lines are not strong, that predictions of the ``Lyman line_12: valley'' may be correct, and that low redshift Ly-alpha is more line_13: prevalent than expected. Observations of low redshift QSOs (including line_14: 3C 273) have shown even more clearly that Ly-alpha absorption occurs line_15: in greater numbers than expected, as well as showing emission--line line_16: profile differences more clearly than from earlier data. line_17: Unexpectedly, Ly-alpha is narrower than H-alpha. ! question: 9 section: 2 line_1: ``HST Imaging of the Inner 3 Arcseconds of NGC 1068 in the Light of [O line_2: III] lambda5007'', I.N.Evans, H.C.Ford, A.L.Kinney, R.R.J.Antonucci, line_3: L.Armus, and S.Caganoff, {\it Ap.J.(Lett.)}, {\bf 369}, L27, 1991. line_4: ``Faint Object Camera Observations of a Globular Cluster Nova Field'', line_5: B.Margon, S.F.Anderson, R.A.Downes, R.C.Bohlin, and P.Jakobsen, {\it line_6: Ap.J.(Lett.)}, {\bf 369}, L71, 1991. line_7: ``Far--Ultraviolet Spectroscopy of the Quasar UM 675 with the Faint line_8: Object Spectrograph on the Hubble Space Telescope'', E.A.Beaver, line_9: E.M.Burbidge, R.D.Cohen, V.T.Junkkarinen, R.W.Lyons, E.I.Rosenblatt, line_10: G.F.Hartig, B.Margon, and A.F.Davidsen, {\it Ap.J.(Lett.)}, {\bf 377}, line_11: L1, 1991. line_12: ``The Ultraviolet Absorption Spectrum of 3C 273'', J.N.Bahcall, line_13: B.T.Jannuzi, D.P.Schneider, G.F.Hartig, R.Bohlin, and V.Junkkarinen, line_14: {\it Ap.J.(Lett.)}, {\bf 377}, L5, 1991. line_15: ``Faint Object Spectrograph Spectroscopy of Resolved Structure in the line_16: Nucleus of NGC 1068'', S.Caganoff, R.R.J.Antonucci, H.C.Ford, line_17: G.A.Kriss, G.Hartig, L.Armus, I.N.Evans, E.Rosenblatt, R.C.Bohlin, and line_18: A.L.Kinney, {\it Ap.J.(Lett.)}, {\bf 377}, L9, 1991. line_19: ``Faint Object Spectrograph Observations of the Low-Luminosity Seyfert line_20: Galaxy NGC 1566'', G.A.Kriss, G.F.Hartig, L.Armus, W.P.Blair, line_21: S.Caganoff, and L.Dressel, {\it Ap.J.(Lett.)}, {\bf 377}, L13, 1991. ! question: 10 section: 1 line_1: The majority of the resources required for this project other than the line_2: normal facilities of a university (librarys, offices, etc.) were line_3: supplied by NASA to the members of the FOS IDT for these projects. line_4: These include all the computing facilities required for the completion line_5: of data reduction and analysis. line_6: Optical and IR ground--based observing facilities and support are line_7: provided by the University of California. ! question: 13 section: 1 line_1: We will observe 2 cases of gravitationally lensed QSOs to investigate line_2: faint additional images and size of clouds producing absorption. ! !end of general form text general_form_address: lname: BURBIDGE fname: E. MARGARET category: PI inst: UNIVERSITY OF CALIFORNIA, SAN DIEGO addr_1: CASS 0111, UCSD addr_2: 9500 GILMAN DRIVE city: LA JOLLA state: CA zip: 920930111 country: USA phone: 619-534-4477 ! ! end of general_form_address records fixed_targets: targnum: 4 name_1: PG1115+080A descr_1: E,313,323,321,923, descr_2: H,515,519 pos_1: RA = 11H 18M 16.934S +/- 1.0", pos_2: DEC = 07D 45' 58.53" +/- 1.0", pos_3: PLATE-ID = 00ZW, pos_4: TBD-EARLY equinox: 2000 pm_or_par: NO rv_or_z: Z=1.722 acqpr_1: COMP comment_1: EXACT COORDINATES WILL BE DEFINED comment_2: FROM WFC IMAGES TAKEN BY WF/PC TEAM comment_3: THE BRIGHTEST IMAGE OF THIS comment_4: MULTIPLE QUASAR. fluxnum_1: 1 fluxval_1: V=17.0 +/- 1.0 fluxnum_2: 2 fluxval_2: F(1500)=2.0 +/- 0.5 E-15 ! targnum: 7 name_1: PG1115+080D descr_1: E,313,323,321,923, descr_2: H,515,519 pos_1: R = 0.50" +/- 0.03", pos_2: PA = 25D +/- 10D, pos_3: FROM 4, TBD-EARLY, pos_4: PLATE-ID = 00ZW, equinox: 2000 pm_or_par: NO rv_or_z: Z=1.722 acqpr_1: COMP comment_1: EXACT OFFSETS FROM -OFFSET WILL BE comment_2: MEASURED FROM WFC IMAGE comment_3: THE SECOND BRIGHTEST IMAGE OF THIS comment_4: MULTIPLE QUASAR. fluxnum_1: 1 fluxval_1: V=17.3 +/- 1.0 fluxnum_2: 2 fluxval_2: F(1500)=2.0 +/- 0.5 E-15 ! targnum: 14 name_1: PG1115+080A-OFFSET descr_1: A,137 pos_1: RA = 11H 18M 16.934S +/- 1.0', pos_2: DEC = 07D 45' 58.53" +/- 1.0', pos_3: PLATE-ID = 00ZW, pos_4: TBD-EARLY equinox: 2000 pm_or_par: NO comment_1: NUMBER 3 ON OUR CHART comment_2: EXACT OFFSETS FOR THE QSOS WILL BE comment_3: MEASURED SHORTLY FROM WFC IMAGE fluxnum_1: 1 fluxval_1: B=16.3 +/- 1.5 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 18.580 targname: PG1115+080A-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 11S fluxnum_1: 1 priority: 1 param_1: BRIGHT = 238313 req_1: ONBOARD ACQ FOR 18.59-18.9; req_2: SEQ 18.58-18.9 NO GAP; req_3: REQ UPDATE ! linenum: 18.590 targname: PG1115+080A config: FOS/RD opmode: ACQ aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 11S fluxnum_1: 1 priority: 1 req_1: REQ UPDATE; ! linenum: 18.600 targname: PG1115+080A config: FOS/RD opmode: RAPID aperture: 0.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 5050S s_to_n: 15 fluxnum_1: 2 priority: 1 param_1: READ-TIME=40 req_1: REQ UPDATE ! linenum: 18.700 targname: PG1115+080A config: FOS/RD opmode: RAPID aperture: 0.3 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 5074S s_to_n: 15 fluxnum_1: 2 priority: 1 param_1: READ-TIME=40 req_1: REQ UPDATE ! linenum: 18.900 targname: PG1115+080A config: FOS/RD opmode: RAPID aperture: 0.3 sp_element: G400H wavelength: 4000 num_exp: 1 time_per_exp: 2400S s_to_n: 15 fluxnum_1: 2 priority: 1 param_1: READ-TIME=40 req_1: REQ UPDATE ! linenum: 22.000 targname: PG1115+080A-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 11S fluxnum_1: 1 priority: 1 param_1: BRIGHT = 238313 req_1: ONBOARD ACQ FOR 22.5-25; req_3: SEQ 22-25 NO GAP; req_6: CYCLE 9 / 18.58-25; req_7: REQ UPDATE comment_1: DO A BLIND OFFSET FROM THIS STAR TO comment_2: PG1115+080D. THE OFFSET WILL BE comment_3: DETERMINED FROM THE WFC IMAGES ! linenum: 22.500 targname: PG1115+080D config: FOS/RD opmode: ACQ aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 11S fluxnum_1: 1 priority: 1 req_1: REQ UPDATE; ! linenum: 23.000 targname: PG1115+080D config: FOS/RD opmode: RAPID aperture: 0.3 sp_element: G400H wavelength: 4000 num_exp: 1 time_per_exp: 3100S s_to_n: 15 fluxnum_1: 2 priority: 1 param_1: READ-TIME=40 req_1: REQ UPDATE; ! linenum: 24.000 targname: PG1115+080D config: FOS/RD opmode: RAPID aperture: 0.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 6820S s_to_n: 15 fluxnum_1: 2 priority: 1 param_1: READ-TIME=40 req_1: REQ UPDATE; ! linenum: 25.000 targname: PG1115+080D config: FOS/RD opmode: RAPID aperture: 0.3 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 7337S s_to_n: 15 fluxnum_1: 2 priority: 1 param_1: READ-TIME=40 req_1: REQ UPDATE; ! ! end of exposure logsheet ! No scan data records found